<b>Abstract</b>— <p>Observations show that situations sometimes arise when the solar wind, which is super-Alfvénic where the planets of the Solar System are located, becomes sub-Alfvénic in the orbit of Mercury and even at 1 AU. The work considers the event described in detail in the article (Bowers et al., 2025), which occurred on May 1, 2013, when a coronal mass ejection that reached Mercury simulated a sub-Alfvénic flow of magnetized solar wind plasma. At the same time, a strong interplanetary magnetic field (IMF) was directed towards the Sun and towards the dawn. In this case, we used a semiempirical modified paraboloid model to present the changes in Mercury’s magnetosphere. The results of the calculations were compared with the calculations in the MHD-model in the work (Bowers et al., 2025) for super-Alfvénic and sub-Alfvénic flow regimes. A good correspondence between the calculations in these two models was obtained and a new effect of the possible splitting of the Alfvén wings, caused by the presence of neutral points of the magnetic field in the cusps and in the tail in the paraboloid model of the magnetosphere, was revealed.</p>